Modelling magnetic flux emergence in the solar convection zone

TL;DR

This study uses 3D magnetohydrodynamic simulations to explore how magnetic flux tubes emerge in the solar convection zone, highlighting the roles of magnetic buoyancy, tube strength, and initial conditions.

Contribution

It provides new insights into the flux emergence process by systematically analyzing the effects of initial magnetic field strength, tube width, and Reynolds number in a convective environment.

Findings

Stronger flux tubes resist convective disruption better.

Magnetic buoyancy enhances flux emergence in strong field cases.

Flux emergence rates decrease with higher magnetic Reynolds numbers.

Abstract

[Abridged] Bipolar magnetic regions are formed when loops of magnetic flux emerge at the solar photosphere. Our aim is to investigate the flux emergence process in a simulation of granular convection. In particular we aim to determine the circumstances under which magnetic buoyancy enhances the flux emergence rate (which is otherwise driven solely by the convective upflows). We use three-dimensional numerical simulations, solving the equations of compressible magnetohydrodynamics in a horizontally-periodic Cartesian domain. A horizontal magnetic flux tube is inserted into fully developed hydrodynamic convection. We systematically vary the initial field strength, the tube thickness, the initial entropy distribution along the tube axis and the magnetic Reynolds number. Focusing upon the low magnetic Prandtl number regime (Pm<1) at moderate magnetic Reynolds number, we find that the flux tube is always susceptible to convective disruption to some extent. However, stronger flux tubes tend to maintain their structure more effectively than weaker ones. Magnetic buoyancy does enhance the flux emergence rates in the strongest initial field cases, and this enhancement becomes more pronounced when we increase the width of the flux tube. This is also the case at higher magnetic Reynolds numbers, although the flux emergence rates are generally lower in these less dissipative simulations because the convective disruption of the flux tube is much more effective in these cases. These simulations seem to be relatively insensitive to the precise choice of initial conditions: for a given flow, the evolution of the flux tube is determined primarily by the initial magnetic field distribution and the magnetic Reynolds number.